We present N2H+ (J arrow 1-0) maps of the dense
gas surrounding three active star formation regions in the
Chamaeleon I and II dark cloud complexes. In each region, we
find 1-5 M\odot of quiescent dense gas organized in
clumps or groups of connected clumps, with a typical size of
0.05 pc. In one region (CHA-Ia), a deeply embedded forming
star is located at the center of the N2H+ core, while
in the other two regions, the forming stars and dense cores
are not as precisely aligned. The small measured line widths
(\Delta VFWHM ~0.4 km s-1) and low excitation
temperatures inferred from the N2H+ emission indicate
that the star formation activity has not injected
substantial kinetic energy into the core material, and
therefore we conclude that these dense cores are attractive
sites for continued and future star formation. We also
present 12CO (J arrow 1-0) maps toward each of
these regions, and identify low-velocity bipolar outflows
from two of the three regions. We identify the deeply
embedded source CHA-MMS1 as the driving source of the
outflow in the CHA-Ia region, and suggest that this source
may also be responsible for the Herbig-Haro objects HH 49-50
and possibly HH 51. This research was supported by grants
PHY0097424 and AST037530 from the US National Science
Foundation.